Black holes are solutions to Einstein's equation in different scenarios[1]}, [2]}, [3]}. These solutions play important role in high energy physics and astrophysics. The fundamental role of these solutions makes it highly important to study the nature of their stability under linear perturbations of different spins. In this context one considers a test wave impinging on a black hole, a part of which is reflected by the effective potential (felt by it) and scattered to infinity. The transmitted part is swallowed by the black hole. Thus, it is expected that the amplitude of the outgoing wave is smaller than that of the incident wave. It was shown that the Schwarzschild black hole is stable under all kind of massless perturbation [4]}, [5]}, [6]}, [7]}. On the other hand, the stability issue of the rotating black holes is more complicated due to the presence of ergoregion outside the event horizon. In this region the conserved energy of causal matter become negative. One can utilize this fact to extract the rest energy and rotational energy of the black hole[8]}, [9]}, [10]}. It is shown [11]}, [12]} that when a bosonic wave impinges on a Kerr-like black hole, the reflected wave can be amplified if the so-called superradiance condition [1]} is satisfied. In this case, the wave near the horizon becomes outgoing [12]} and extracts rotational energy of black hole from the ergosphere. If this process continues to occur then a Kerr-black hole finally becomes a Schwarzschild black hole. Due to the Pauli exclusion principle, such phenomena is absent in the case of fermionic scattering[11]}.
